HR: 1340h
AN: SH53A-1236    [Abstracts]
TI: Simulating Coupling Complexity in Space Plasmas: First Results from a new code
AU: Kryukov, I
EM: kryukov@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: * Zank, G P
EM: zank@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Pogorelov, N V
EM: nikolai.pogorelov@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Raeder, J
EM: J.Raeder@unh.edu
AF: Space Science Institute, University of New Hampshire, Durham, NH 03824 United States
AU: Ciardo, G
EM: ciardo@cs.ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Florinski, V A
EM: vflorins@citrus.ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Heerikhuisen, J
EM: jacobh@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Li, G
EM: gang.li@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Petrini, F
EM: fabrizio@lanl.gov
AF: Los Alamos National Lab, Los Alamos National Lab, Los Alamos, NM 87545 United States
AU: Shematovich, V I
EM: shematov@inasan.rssi.ru
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Winske, D
EM: winske@lanl.gov
AF: Los Alamos National Lab, Los Alamos National Lab, Los Alamos, NM 87545 United States
AU: Shaikh, D
EM: dastgeer@citrus.ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Webb, G M
EM: gmwebb@ucr.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 United States
AU: Yee, H M
EM: yee@nas.nasa.gov
AF: NASA Ames Research Center, NASA Ames Research Center, Moffett Field, CA 94035 United States
AB: The development of codes that embrace 'coupling complexity' via the self-consistent incorporation of multiple physical scales and multiple physical processes in models has been identified by the NRC Decadal Survey in Solar and Space Physics as a crucial necessary development in simulation/modeling technology for the coming decade. The National Science Foundation, through its Information Technology Research (ITR) Program, is supporting our efforts to develop a new class of computational code for plasmas and neutral gases that integrates multiple scales and multiple physical processes and descriptions. We are developing a highly modular, parallelized, scalable code that incorporates multiple scales by synthesizing 3 simulation technologies: 1) Computational fluid dynamics (hydrodynamics or magneto-hydrodynamics-MHD) for the large-scale plasma; 2) direct Monte Carlo simulation of atoms/neutral gas, and 3) transport code solvers to model highly energetic particle distributions. We are constructing the code so that a fourth simulation technology, hybrid simulations for microscale structures and particle distributions, can be incorporated in future work, but for the present, this aspect will be addressed at a test-particle level. This synthesis we will provide a computational tool that will advance our understanding of the physics of neutral and charged gases enormously. Besides making major advances in basic plasma physics and neutral gas problems, this project will address 3 Grand Challenge space physics problems that reflect our research interests: 1) To develop a temporal global heliospheric model which includes the interaction of solar and interstellar plasma with neutral populations (hydrogen, helium, etc., and dust), test-particle kinetic pickup ion acceleration at the termination shock, anomalous cosmic ray production, interaction with galactic cosmic rays, while incorporating the time variability of the solar wind and the solar cycle. 2) To develop a coronal mass ejection and interplanetary shock propagation model for the inner and outer heliosphere, including, at a test-particle level, wave-particle interactions and particle acceleration at traveling shock waves and compression regions. 3) To develop an advanced Geospace General Circulation Model (GGCM) capable of realistically modeling space weather events, in particular the interaction with CMEs and geomagnetic storms. Furthermore, by implementing scalable run-time supports and sophisticated off- and on-line prediction algorithms, we anticipate important advances in the development of automatic and intelligent system software to optimize a wide variety of 'embedded' computations on parallel computers. Finally, public domain MHD and hydrodynamic codes had a transforming effect on space and astrophysics. We expect that our new generation, open source, public domain multi-scale code will have a similar transformational effect in a variety of disciplines, opening up new classes of problems to physicists and engineers alike.
DE: 7833 Mathematical and numerical techniques (0500, 3200)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005